We then fitted this eclipse light curve using version 42 of the jktebop\(\endcsname \)http://www.astro.keele.ac.uk/jkt/codes/jktebop.html
 code [1]}, [2]}. We fitted for the orbital period (\(P\) ) and time of mid-eclipse (\(T_0\) ), the sum (\(r_{\rm A}+r_{\rm B}\) ) and ratio (\(k = {r_{\rm B}}/{r_{\rm A}}\) ) of the fractional radii, the orbital inclination (\(i\) ), and the central surface brightness ratio of the two stars (\(J\) ). We adopted a quadratic limb darkening (LD) law, fitted for the linear coefficients for each star (\(u_{\rm A}\)  and \(u_{\rm B}\) ) and fixed the quadratic coefficients (\(v_{\rm A}\)  and \(v_{\rm B}\) ) to theoeretical values from Claret [3]}. A circular orbit was adopted as we found the orbital eccentricity to be extremely small and consistent with zero. Third light was found to be insignificant and typically slightly below zero so was fixed at zero. We term the star eclipsed at the deeper eclipse star A and its companion star B; star A is hotter, larger and more massive than star B.
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